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The Science Verification of FLAMES FRANCESCA PRIMAS, User Support Group, ESO

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The Science Verification of FLAMES FRANCESCA PRIMAS, User Support Group, ESO The Science Verification of FLAMES FRANCESCA PRIMAS, User Support Group, ESO After a new VLT instrument has been sition of UVES and GIRAFFE observa- munity at large) and the proposed ex- commissioned and thoroughly tested1, a tions. ploitation of the instrument capabilities: series of scientific and technical check- The FLAMES Dry Runs took place ups are scheduled in order to test the successfully between the end of • The Chemical Signature of Different front-to-end operations chain before the January and the beginning of February Stellar Populations in the LMC: al- official start of regular operations. (Jan 24 – Feb 03, 2003). Nine science though it is considered an intermediate- Technically speaking, these are the so- programmes, proposed and assembled age galaxy, the LMC is characterised by called Dry Runs, part of which are usu- by the FLAMES SV Team (which in- a large range of stellar ages, from a ally devoted to the Science Verification cluded the VLT Programme Scientist, genuine old to a prominent young pop- (SV for short) of that specific instru- the Instrument PI, the Paranal ulation. The main goal of this project ment. Instrument Scientist, the User Support was to investigate further its metal en- A Science Verification programme in- Astronomer, members of the FLAMES richment history by measuring the cludes a set of typical scientific obser- Commissioning and Science Advisory abundances of several elements for a vations with the aim of verifying and Teams and representatives of the statistically significant sample of Red demonstrating to the community the ca- FLAMES Consortia), were executed. Giant Branch stars (17 < Vmag < 18). pabilities of a new instrument in the op- More than 5200 spectra were collected Two complementary projects were com- erational framework of the VLT Paranal during the ten observing nights, and bined: (1) the first spectroscopic metal- Observatory. Though manifold, its goals publicly released on March 3, exactly licity determination of the LMC Clump to can be summarised in two main points: one month after the last observing verify its influence (if any) on the intrin- from the scientific point of view, by night. This one-month time lag was nec- sic luminosity of the stars (by allocating demonstrating the scientific potential of essary to visually inspect the quality of 1/4 of the Medusa fibres to Clump the new instrument, these observations the frames (both raw and reduced), to stars); (2) the chemical analysis of LMC will provide ESO users with first sci- make the correct association between Long Period Variables in order to inves- ence-grade data, thus fostering an ear- raw and calibration frames to be distrib- tigate the connection (if any) among ly scientific return. From the technical uted, and to prepare a detailed set of their chemical composition, pulsation point of view, by testing the whole oper- summaries and technical explanations. mode, and evolutionary phase (the ational system (from the preparation of Any user from one of the ESO Member UVES fibres were used for this pur- the observations to their execution and States and with an active registration pose). Figure 1 shows the H-α region analysis), it will provide important feed- to the ESO/ST-ECF Archive (see for one RGB, one Clump, and one LPV back to the Instrument Operation http://archive.eso.org/register/new for star. Teams (both in Paranal and in more information), can download the Garching), to the Instrument Division, FLAMES SV datasets, whose scientific • Massive Kinematic Study of and to the Data Flow groups. More de- justifications are briefly described be- NGC 5128 using its Planetary tails about the concept(s) behind a low. The interested reader is reminded Nebulae and Globular Clusters as Science Verification can be found in the that a wealth of details (such as colour- Test Probes: planetary nebulae (PN) “Science Verification Policy and magnitude diagrams - to check which are emission line objects, the systemic Procedures” document (available at targets were observed, Field Charts velocities of which can be probed using http://www.eso.org/science/vltsv/). and README files - two of the main the brightest emission lines (see user requirements) are available Figure 2). The 785 PN found and cata- Science Goals and Achievements from the FLAMES SV web page logued by Hui et al. (1993), over a large (http://www.eso.org/science/vltsv). The area (40҂46 arcmin, EWxNS) of The Fibre Large Array Multi-Element following SV programmes were select- NGC 5128 (Centaurus A) were targeted Spectrograph (FLAMES) is the new ed based on their scientific weight (they in order to verify the initial findings that multi-object, intermediate- and high- must be interesting for the ESO com- PN kinematics trace a triaxial potential, resolution spectrograph of the VLT (Pasquini et al. 2002). Mounted at the Nasmyth A platform of Kueyen (Unit Telescope #2), FLAMES can access targets over a large corrected field of view (25 arcmin diameter). It consists of three main components: a Fibre Positioner (OzPoz) hosting two plates (while one plate is observing, the other is positioning the fibres for the next ob- servation); a link to the Red Arm of UVES (the high-resolution Ultraviolet and Visible Echelle Spectrograph) via 8 single fibres of 1 arcsec entrance aper- Figure 1: The H-α ture; a medium-high resolution optical region as observed spectrograph, GIRAFFE, equipped with with Medusa and three types of feeding fibre systems: UVES (top spec- 130 MEDUSA fibres, 15 deployable in- trum) in three stars tegral field units (IFU), and 1 large, fixed representative of integral field unit (ARGUS). A special the different stellar Observing Software (OS) coordinates populations probed the operation of the different subsys- in the Large tems, also allowing simultaneous acqui- Magellanic Cloud. 1Please note that all commissioning data are now available from http://www.eso.org/science/flames_comm/ 3 Figure 2: H-β and two [O III] lines in emission (the 495.9 and 500.7 nm), as detected in one of the planetary nebula observed with one Medusa fibre, at low resolution. More than 500 PN were observed in total. Figure 3: Two mass-loss diagnostics: the Ca H,K and the NaD lines, as observed in two different RGB stars of NGC 2808. with the mass-to-light ratio increasing •Elemental Abundances in NGC 2243: • Probing Activity and Angular Mo- with radius (thus suggesting the pres- a complete chemical analysis of sub-gi- mentum Evolution of Low-Mass ence of a dark matter halo). Some ant stars and membership information Members of the Orion Nebular MEDUSA and all UVES fibres were al- for the fainter, turn-off stars in this open, Cluster: surface rotation is a key ob- located to the brightest globular clusters metal-poor, intermediate-age (~ 2 Gyr) servational parameter for stellar evolu- of this giant elliptical galaxy in order to cluster were the main goals of the pro- tion, being tightly linked to the internal compare their kinematics and to derive gramme, which used two contiguous angular momentum transport, hence to their metallicity. (hence slightly overlapping) high-reso- mass loss. The main goal of this pro- lution Medusa set-ups (Figure 4). The gramme was to determine the v sini dis- • Mass Loss in Red Giant Stars of main scientific interest of this cluster lies tribution for a large number (120 tar- the Globular Cluster NGC 2808: in two aspects: its metallicity, which is gets, selected from the low-resolution about 100 stars of the Red Giant comparable to the halo cluster 47 survey of Hillenbrand 1997) of low- Branch, in the magnitude interval Tucanae, and its age which is instead mass (0.2–0.06 Mी), relatively cold V=13.2–16.5 mag, within a radius of remarkably smaller (47 Tuc formed (logTeff < 3.5), M5–M7 type stars in the about 7 arcmin from the cluster centre, some 10–12 Gyrs earlier). A direct Orion Nebular Cluster (~1 Myr old, were targeted, with the aim of measur- abundance comparison between these 430 pc away), for which only little infor- ing shifts of the CaII-K3, NaD and H-α two clusters (47 Tucanae has been ex- mation is available. Recent observa- core line profiles that are major diag- tensively observed with UVES in the tions in Orion have shown that while the nostics of mass outflow, hence mass past) will shed light not only on their majority of low-mass pre-main se- loss. In order to observe the Ca H and chemical history, but also on the forma- quence stars are rotating at rates ap- K lines, this programme made use of tion and evolution of our own Galaxy. proaching 30% of breakup, late-type one of the bluest settings available on FLAMES, HR#2, which covers the spectral range between 385 and 405 nm (see Figure 3). The brightest stars of the cluster were observed si- multaneously with UVES, to obtain a larger spectral coverage (480–680 nm) for chemical abundance purposes. • Geometric Distances of the Galactic Globular Cluster NGC 2808: the main idea behind this science case was to observe a very large number of stars (1000), and derive their radial velocities, in order to obtain the first determination of the cluster geometric distance (with an uncertainty of 2–3%, i.e. an age with an error less than 1 Gyr) via a direct comparison of the radial velocities to the (already available) proper motions. One GIRAFFE set-up (HR#5), together with the simultaneous allocation of UVES-fibres, was also used to obtain spectra of horizontal branch stars, thus increasing by one order of magnitude the size of the present sample. Figure 4: The same NGC 2243 sub-giant star, as observed in two contiguous high resolu- tion Medusa settings: the total spectral coverage is from 638 to 697 nm.
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